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<supportEmail caption="Support">icrc2007@icrc2007.unam.mx</supportEmail>
<title>30th International Cosmic Ray Conference</title>
<description>The 30th International Cosmic Ray Conference will be held from July 3, 2007 to July 11, 2007 in Merida, Yucatan, Mexico.</description>
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 <name>Merida, Mexico</name>
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<startDate>2007-07-03T08:00:00</startDate>
<endDate>2007-07-11T19:00:00</endDate>
<creationDate>2005-09-26T05:04:53</creationDate>
<modificationDate>2024-04-12T17:46:55</modificationDate>
<timezone>Mexico/General</timezone>
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 <title>Study of the 27-day variation of the GCR anisotropy based on the experimental data and theoretical modeling</title>
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   <name first="Renata" middle="" last="Modzelewska"></name>
   <organization>Institute of Math. And Physics of University of Podlasie, Siedlce, Poland</organization>
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   <title>Ms.</title>
   <name first="Renata" middle="" last="Modzelewska"></name>
   <organization>Institute of Math. And Physics of University of Podlasie, Siedlce, Poland</organization>
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   <organization>Institute of Math. And Physics of University of Podlasie, Siedlce, Poland, Institute of Geophysics of Academy of Sciences of Georgia, Tbilisi, Georgia</organization>
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  <name>Merida, Mexico</name>
  <address></address>
  <room>Regency (Hyatt)</room>
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 <startDate>2007-07-09T14:45:00</startDate>
 <endDate>2007-07-09T14:45:00</endDate>
 <abstract>We study features of the 27-day variation of the galactic cosmic ray (GCR) three
dimensional anisotropy calculated by the global spherical analyses method (GSM) using
Fourier harmonic frequency filter, Chree’s diagram and epicyclegrams. We found that
the greater amplitudes of the 27-day variation of the GCR anisotropy in the minima
epoch of solar activity for the A&gt;0 polarity period than for the A&lt;0 polarity period
are related with the heliolongitudinal asymmetry of the solar wind velocity. The
continuous background 27-day variation of the GCR anisotropy is observed owing to the
existence of the long-lived 27-day variation of the solar wind velocity, especially
in the minima epoch of solar activity.
We develop 3-D stationary model based on the transport equation of GCR with the 3D
modified Parker’s spiral interplanetary magnetic field. We assume that 27-day
variation of the GCR anisotropy is caused by the heliolongitudinal changes of the
solar wind velocity; in this case solution of the transport equation gives the
results compatible with the neutron monitors experimental data.</abstract>
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